The Collapse of Rotating Massive Stars in Three Dimensions

By Chris L. Fryer, Michael S. Warren. 2003

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Most simulations of the core collapse of massive stars have focused on the collapse of spherically symmetric objects. If these stars are rotating, this symmetry is broken, opening up a number of effects that are just now being studied. The list of proposed effects spans a range of extremes: from fragmentation of the collapsed iron core to modifications of the convective instabilities above the core; from the generation of strong magnetic fields that then drive the supernova explosion to the late-time formation of magnetic fields to produce magnetars after the launch of the supernova explosion. The list of the observational effects of rotation ranges from modifications in the gamma-ray line spectra, nucleosynthetic yields, and shape of supernova remnants caused by rotation-induced asymmetric explosions to strong pulsar radiation, the emission of gravitational waves, and altered r-process nucleosynthetic yields caused by rapidly rotating stars. In this paper we present the results of three-dimensional collapse simulations of rotating stars for a range of stellar progenitors. We find that for the most rapidly spinning stars, rotation does indeed modify the convection above the proto-neutron star, but it is not fast enough to cause core fragmentation. Similarly, although strong magnetic fields can be produced once the proto-neutron star cools and contracts, the proto-neutron star does not spin fast enough to generate strong magnetic fields quickly after collapse, and, for our simulations, magnetic fields will not dominate the supernova explosion mechanism. Even so, the resulting pulsars for our most rapidly rotating models may emit enough energy to dominate the total explosion energy of the supernova. However, more recent stellar models predict rotation rates that are much too slow to affect the explosion, but these models are not sophisticated enough to determine whether the most recent or past stellar rotation rates are more likely. Thus, we must rely on observational constraints to determine the true rotation rates of stellar cores just before collapse. We conclude with a discussion of the possible constraints on stellar rotation that we can derive from core-collapse supernovae.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/75175e50403a61b5aa96ce9c49cbfc2ef4933213

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Citations in the corpus

Stellar evolution with rotation XII. Pre-supernova models (2004, background): “This means that in any case, additional slow down is necessary during the core collapse (Woosley & Heger 2003; Fryer & Warren 2004) in order to reproduce the observed rotation periods of young pulsars.”
Non-spherical core collapse supernovae - II. The late-time evolution of globally anisotropic neutrino-driven explosions and their implications for SN 1987 A (2005, background): “…2D simulations, which include spectral neutrino transport, (see Buras et al. 2003, 2006a,b) could not confirm the success of first generation models, which employed gray neutrino diffusion and found explosions (e.g. Herant et al. 1994; Burrows et al. 1995; Fryer 1999; Fryer & Warren 2002, 2004).”
DELAYED NEUTRINO-DRIVEN SUPERNOVA EXPLOSIONS AIDED BY THE STANDING ACCRETION-SHOCK INSTABILITY (2007, background): “…vigorous than in previous multi-dimensional models with a grey neutrino diffusion scheme (e.g., Herant et al. 1994; Burrows et al. 1995; Fryer 1999; Fryer & Warren 2002, 2004), mainly because the accretion shock in the new models lingers at rather small radii and the correspondingly high infall…”
The Spin Periods and Rotational Profiles of Neutron Stars at Birth (2005, background): “In their recent gray, three-dimensional smoothed particle radiation-hydrodynamics calculation, Fryer & Warren (2004) estimated neutron star spin periods by assuming that the angularmomentumof the inner 1M is conserved as the PNS cools and contracts to a neutron star.”
Postbounce Evolution of Core-Collapse Supernovae: Long-Term Effects of the Equation of State (2005, background): “…with approximate neutrino-transport schemes have revealed the importance of asymmetry such as rotation, convection, magnetic fields and/or hydrodynamical instability (Blondin et al. 2003; Buras et al. 2003; Kotake et al. 2003; Fryer & Warren 2004; Kotake et al. 2004; Walder et al. 2004).”
THREE-DIMENSIONAL CORE-COLLAPSE SUPERNOVA SIMULATED USING A 15 M⊙ PROGENITOR (2015, background): “Earlier work by Fryer & Warren (2002, 2004) using non-spectral νRHD found explosions in 2D and 3D to be similar.”
THE LANDSCAPE OF THE NEUTRINO MECHANISM OF CORE-COLLAPSE SUPERNOVAE: NEUTRON STAR AND BLACK HOLE MASS FUNCTIONS, EXPLOSION ENERGIES, AND NICKEL YIELDS (2014, background): “…and in the heating region between the PNS and the shock (Herant et al. 1992, 1994; Janka & Mueller 1996; Burrows et al. 1995; Fryer & Heger 2000; Fryer & Warren 2002, 2004; Buras et al. 2006; Murphy & Meakin 2011; Burrows et al. 2012; Murphy et al. 2013; Ott et al. 2013), the standing accretion…”
Viscosity and Rotation in Core-Collapse Supernovae (2004, methodology): “We find a similar magnitude change in j at this value of M, implying that the magnitude of the intrinsic angular momentum transport in the simulations of Fryer & Warren (2004) is comparable to the transport caused here by our explicit viscosity.”
Constraints from Gravitational-wave Detections of Binary Black Hole Mergers on the 12C(α, γ)16O Rate (2020, background): “Rotation may play a role in the final black hole mass, depending on how material with high angular momentum is accreted onto the black hole during the collapse (Fryer & Warren 2004; Rockefeller et al. 2006; Batta et al. 2017).”
Two-Dimensional Multiangle, Multigroup Neutrino Radiation-Hydrodynamic Simulations of Postbounce Supernova Cores (2008, background): “The fact that 2D gray FLD schemes have in the past led to neutrino-driven explosions (Herant et al. 1994; Burrows et al. 1995; Fryer & Heger 2000; Fryer & Warren 2002, 2004), while MGFLD schemes appear not to (Walder et al. 2005; Burrows et al. 2006, 2007c), emphasizes the importance of a spectral…”
Neutrino-dominated Accretion and Supernovae (2005, background): “341 et al. 2004; Walder et al. 2005 and references therein) and even three dimensions (Fryer & Warren 2004; Janka et al. 2004).”
The Supernova Gamma-Ray Burst Connection (2006, background): “It may be that the neutron star models require the initial operation of a successful neutrino-powered explosion before they can function (Fryer and Warren, 2004).”